Lecture 34 Scattering of Electromagnetic Field

Lecture 34 Scattering of Electromagnetic Field The scattering of electromagnetic field is an important topic. A source radiates a field, and ultimately, in the far field of the source, the field resembles a plane wave. When a plane wave impinges on an object or a scatterer, the energy carried by the plane wave is deflected to other directions which is the process of scattering. In the optical regime, the scattered light allows us to see objects, as well as admire all hues that are observed of objects. In microwave, the scatterers cause the loss of energy carried by a plane wave. A proper understanding of scattering theory allows us to understand many physical phenomena around us. We will begin by studying Rayleigh scattering, which is a way to study scattering by small objects. 34.1 Rayleigh Scattering Rayleigh scattering is a solution to the scattering of light by small particles. These particles are assumed to be much smaller than wavelength of light. Then a simple solution can be found by the method of asymptotic matching. This single scattering solution can be used to explain a number of physical phenomena in nature. For instance, why the sky is blue, the sunset so magnificently beautiful, how birds and insects can navigate themselves without the help of a compass. By the same token, it can also be used to explain why the Vikings, as a seafaring people, could cross the Atlantic Ocean over to Iceland without the help of a magnetic compass. 333 334 Electromagnetic Field Theory Figure 34.1: The magnificent beauty of nature can be partly explained by Rayleigh scattering [196, 197]. When a ray of light impinges on an object, we model the incident light as a plane electromagnetic wave (see Figure 34.2). Without loss of generality, we can assume that the electromagnetic wave is polarized in the z direction and propagating in the x direction. We assume the particle to be a small spherical particle with permittivity "s and radius a. Essen- tially, the particle sees a constant field as the plane wave impinges on it. In other words, the particle feels an almost electrostatic field in the incident field. Figure 34.2: Geometry for studying the Rayleigh scattering problem. Scattering of Electromagnetic Field 335 34.1.1 Scattering by a Small Spherical Particle The incident field polarizes the particle making it look like an electric dipole. Since the incident field is time harmonic, the small electric dipole will oscillate and radiate like a Hertzian dipole in the far field. First, we will look at the solution in the vicinity of the scatterer, namely, in the near field. Then we will motivate the form of the solution in the far field of the scatterer. (Solving a boundary value problem by looking at the solutions in two different physical regimes, and then matching the solutions together is known as asymptotic matching.) A Hertzian dipole can be approximated by a small current source so that J(r) =zIlδ ^ (r) (34.1.1) In the above, we can let the time-harmonic current I = dq=dt = j!q, then Il = j!ql = j!p (34.1.2) where the dipole moment p = ql. The vector potential A due to a Hertzian dipole, after substituting (34.1.1), is ¦ 0 µ 0 J(r ) −jβjr−r0j A(r) = dr 0 e 4π V jr − r j µIl =z ^ e−jβr (34.1.3) 4πr where we have made use of the sifting property of the delta function in (34.1.1) when it is substituted into the above integral. Near Field From prior knowledge, we know that the electric field is given by E = −j!A − rΦ. From dimensional analysis, the scalar potential term dominates over the vector potential term in the near field of the scatterer. Hence, we need to derive, for the corresponding scalar potential, the approximate solution. The scalar potential Φ(r) is obtained from the Lorenz gauge that r · A = −j!µεΦ. Therefore, −1 Il @ 1 Φ(r) = r · A = − e−jβr (34.1.4) j!µε j!"4π @z r When we are close to the dipole, by assuming that βr 1, we can use a quasi-static approximation about the potential.1 Then @ 1 @ 1 @r @ 1 z 1 e−jβr ≈ = = − (34.1.5) @z r @z r @z @r r r r2 1This is the same as ignoring retardation effect. 336 Electromagnetic Field Theory or after using that z=r = cos θ, ql Φ(r) ≈ cos θ (34.1.6) 4π"r2 which is the dipole potential. This dipole induced in the small particle is formed in response to the incident field. The scattered field from the small particle is due to a small induced dipole, and it has a potential given by the previous expression. The incident field can be approximated by a constant local static electric field, Einc =zE ^ i (34.1.7) The corresponding electrostatic potential for the incident field is then2 Φinc = −zEi (34.1.8) so that Einc ≈ −∇Φinc =zE ^ i, as ! ! 0. The scattered dipole potential from the spherical particle in the vicinity of it is given by a3 ql Φ = E cos θ = cos θ (34.1.9) sca s r2 4π"r2 which is the potential due to a static dipole. The electrostatic boundary value problem (BVP) has been previously solved and3 "s − " Es = Ei (34.1.10) "s + 2" Using (34.1.10) in (34.1.9), and comparing with(34.1.6), one can see that the dipole moment induced by the incident field is that "s − " 3 p = ql = 4π" a Ei (34.1.11) "s + 2" Far Field In the far field of the Hertzian dipole, we can start with 1 E = −j!A − rΦ = −j!A − rr · A (34.1.12) j!µε But when we are in the far field, A behaves like a spherical wave which in turn behaves like a local plane wave if one goes far enough. Therefore, r ! −jβ = −jβr^. Using this approximation in (34.1.12), we arrive at ββ E = −j! A − · A = −j!(A − r^r^ · A) = −j!(θA^ + φA^ ) (34.1.13) β2 θ φ where we have usedr ^ = β/β. 2It is not easier to get here from electrodynamics. One needs vector spherical harmonics [198]. 3It was one of the homework problems. Scattering of Electromagnetic Field 337 34.1.2 Scattering Cross Section From (34.1.3), and making use of (34.1.2), we see that Aφ = 0 while j!µql A = − e−jβr sin θ (34.1.14) θ 4πr Consequently, using (34.1.11) for ql, we have in the far field that4 2 3 ∼ ! µql −jβr 2 "s − " a −jβr Eθ = −j!Aθ = − e sin θ = −! µε Eie sin θ (34.1.15) 4πr "s + 2" r r " 1 H =∼ E = E (34.1.16) φ µ θ η θ where η = pµ/ε. The time-averaged Poynting vector is given by hSi = 1=2<e fE × H∗g. Therefore, the total scattered power is obtained by integrating the power density over a spherical surface when r tends to infity. Thus, the total scattered power is ¢ ¢ ¢ ¢ 1 π 2π 1 π 2π P = r2 sin θdθ dφE H∗ = r2 sin θdθ dφjE j2 (34.1.17) s 2 θ φ 2η θ 0 0 ¢ 0 0 2 6 π 1 4 "s − " a 2 2 3 = β 2 jEij r sin θdθ 2π (34.1.18) 2η "s + 2" r 0 But ¢ ¢ ¢ π π π sin3 θdθ = − sin2 θd cos θ = − (1 − cos2 θ)d cos θ 0 0 ¢0 −1 4 = − (1 − x2)dx = (34.1.19) 1 3 Therefore 2 4π "s − " 4 6 2 Ps = β a jEij (34.1.20) 3η "s + 2"s The scattering cross section is the effective area of a scatterer such that the total scattered power is proportional to the incident power density times the scattering cross section. As such it is defined as P 8πa2 " − " 2 Σ = s = s (βa)4 (34.1.21) s 1 2 2η jEij 3 "s + 2" In other words, Ps = hSinci × Σs 4The !2 dependence of the following function implies that the radiated electric field in the far zone is proportional to the acceleration of the charges on the dipole. 338 Electromagnetic Field Theory It is seen that the scattering cross section grows as the fourth power of frequency since β = !=c. The radiated field grows as the second power because it is proportional to the acceleration of the charges on the particle. The higher the frequency, the more the scattered power. this mechanism can be used to explain why the sky is blue. It also can be used to explain why sunset has a brilliant hue of red and orange. The above also explain the brilliant glitter of gold plasmonic nano-particles as discovered by ancient Roman artisans. For gold, the medium resembles a plasma, and hence, we can have "s < 0, and the denominator can be very small. Furthermore, since the far field scattered power density of this particle is 1 hSi = E H∗ ∼ sin2 θ (34.1.22) 2η θ φ the scattering pattern of this small particle is not isotropic. In other words, these dipoles radiate predominantly in the broadside direction but not in their end-fire directions. Therefore, insects and sailors can use this to figure out where the sun is even in a cloudy day. In fact, it is like a rainbow: If the sun is rising or setting in the horizon, there will be a bow across the sky where the scattered field is predominantly linearly polarized.5 Such a \sunstone" for direction finding is shown in Figure 34.3.

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